Calathus: A sample-return mission to Ceres

Ceres, as revealed by NASA's Dawn spacecraft, is an ancient, crater-saturated body dominated by low-albedo clays. Yet, localised sites display a bright, carbonate mineralogy that may be as young as 2 Myr. The largest of these bright regions (faculae) are found in the 92 km Occator Crater, and would have formed by the eruption of alkaline brines from a subsurface reservoir of fluids. The internal structure and surface chemistry suggest that Ceres is an extant host for a number of the known prerequisites for terrestrial biota, and as such, represents an accessible insight into a potentially habitable “ocean world”. In this paper, the case and the means for a return mission to Ceres are outlined, presenting the Calathus mission to return to Earth a sample of the Occator Crater faculae for high-precision laboratory analyses. Calathus consists of an orbiter and a lander with an ascent module: the orbiter is equipped with a high-resolution camera, a thermal imager, and a radar; the lander contains a sampling arm, a camera, and an on-board gas chromatograph mass spectrometer; and the ascent module contains vessels for four cerean samples, collectively amounting to a maximum 40 g. Upon return to Earth, the samples would be characterised via high-precision analyses to understand the salt and organic composition of the Occator faculae, and from there to assess both the habitability and the evolution of a relict ocean world from the dawn of the Solar System.The attached document is the authors’ final accepted version of the journal article provided here with a Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) Creative Commons Licence. You are advised to consult the publisher’s version if you wish to cite from it.

The Case Against Vast Glaciation in Valles Marineris, Mars

The Valles Marineris of Mars form the largest system of interconnected canyons in the Solar System, where morphological, mineralogical, and structural evidence of widespread glaciation has been recently reported. However, neither precipitation models nor global water budgets can account for such a colossal fill, and the hypothesis has thus far remained unchallenged by additional scrutiny. Here, we present the first thorough case against a Valles Marineris glaciation by describing new evidence that precludes the existence of a glacier. Most crucially, we review High Resolution Imaging Science Experiment (HiRISE) images of chaos terrain in Candor Chasma — previously interpreted as remnant glacial ice — and identify layered, boulder-rich scarps bearing no similarity to scarps of massive ice in Promethei Terra or the North Polar Layered Deposits. We also find no significant differences in the structure, morphology, and composition of chaos terrain in Candor and the Chryse Planitia region, which suggests Candor's chaos, like Chryse's, is fractured highland terrain. We also review several other key supports for the glacial hypothesis, including the coincidence of an apparent glacial trimline with the water-bearing mineral jarosite, and the apparent presence of glacial features including kettle holes and sandur plains. These too are found to have more plausible explanations with non-glacial origins including tectonic reorganisation, groundwater sapping, and chaotic fracturing. We conclude that the Valles Marineris glacial hypothesis is inconsistent with both observed morphology and our understanding of the ancient Martian climate, and we find no evidence to support its existence

Use of penetrating GNSS signals for measuring soil moisture

This work introduces a novel approach for soil moisture estimation, based on the measurement of GNSS signals penetrating a soil volume. A model relating soil moisture content (SMC) to the measured soil transmissivity is proposed. The measurement concept is described and a preliminary experimental setup is proposed. The feasibility of the approach is evaluated through simulations of the measured ('apparent') transmissivity as a function of moisture content, surface roughness and receiving antenna depth, among other relevant parameters